ИСТИНА

The astrophysical r-process of nucleosynthesis is widely considered to explain the production of major amount of nuclei beyond the iron peak. This nu- cleosynthesis mechanism poses great interest to both astrophysics and nuclear physics. Taking place at temperatures above 1 GK and very high densities, it is believed to occur in extreme astrophysical scenarios, such as neutron star mer- gers and supernova blasts. Thus the main approach in r-process study is comput- er simulation. Nuclei that take part in r-process reaction chains are exotic due to high neutron excess. To get their characteristics required by nucleosynthesis simula- tions theoretical nuclear models are used. We study the impact of the nuclear mass model choice on the results of r-process calculation. Using three different theoretical mass tables we have created three libraries of astrophysical nuclear reactions based on REACLIB database. We used them to simulate r- process in neutron star merger dynamical ejecta with the help of the SkyNet library. Obtained results show how our r-process simulation responds to the mass model variation.